Hans Baehr, Max-Planck Institut für Astronomie Heidelberg - 14.11.16
Abstract:
The majority of observed planets can be said to have been formed through a 'cold start' process, core accretion. The exception to this are planet observed outside ~30 AU, the existence of which are difficult to reconcile with the slow formation times of core accretion at wide orbits. To explain these objects, gravitational instability (aka disk fragmentation) provides a convenient mechanism which can form these planets. Gravitational instability (GI) is able to form gas giant planets quickly and predominantly in wide orbits. My research focuses on understanding the role self-gravitating phase plays in disk evolution and planet formation, attempting to determine what role GI play in planet formation, whether it complements or competes with core accretion and if we can distinguish between the two.
